1. 4 Mar 08Feng 1 DARK MATTERS CaJAGWR Caltech-JPL 4 March 2008 Jonathan Feng UC Irvine

2. 4 Mar 08Feng 2 Remarkable agreement Dark Matter: 23% ± 4% Dark Energy: 73% ± 4% Baryons: 4% ± 0.4% Neutrinos: 0.2% (  m /0.1eV) Remarkable precision Remarkable results COSMOLOGY NOW

3. 4 Mar 08Feng 3 OPEN QUESTIONS DARK MATTER –Is it a fundamental particle? –What are its mass and spin? –How does it interact? –Is it absolutely stable? –What is the symmetry origin of the dark matter particle? –Is dark matter composed of one particle species or many? –How and when was it produced? –Why does  DM have the observed value? –What was its role in structure formation? –How is dark matter distributed now? DARK ENERGY –What is it? –Why not   ~ 10 120 ? –Why not   = 0? –Does it evolve? BARYONS –Why not  B ≈ 0? –Related to neutrinos, leptonic CP violation? –Where are all the baryons?

4. 4 Mar 08Feng 4 THE DARK UNIVERSE DARK MATTER The problems appear to be completely different No known particles contribute Probably tied to M weak ~ 100 GeV Several compelling solutions DARK ENERGY All known particles contribute Probably tied to M Planck ~ 10 19 GeV No compelling solutions

5. 4 Mar 08Feng 5 Known DM properties DARK MATTER Not baryonic Unambiguous evidence for new physics Not hot Not short-lived Gravitationally interacting

6. 4 Mar 08Feng 6 DARK MATTER CANDIDATES The observational constraints are no match for the creativity of theorists Masses and interaction strengths span many, many orders of magnitude, but not all candidates are equally motivated HEPAP/AAAC DMSAG Subpanel (2007)

7. 4 Mar 08Feng 7 NEW PARTICLES AND NATURALNESS m h ~ 100 GeV,  ~ 10 19 GeV  cancellation of 1 part in 10 34 At ~ 100 GeV we expect new particles: supersymmetry, extra dimensions, something! Classical =+ = − Quantum e + Quantum new particle −

8. 4 Mar 08Feng 8 THE “WIMP MIRACLE” (1)Assume a new (heavy) particle  is initially in thermal equilibrium:  ↔  f f (2) Universe cools:   f f (3)  s “freeze out”:  f f (1) (2) (3) → ← / → ← / / Zeldovich et al. (1960s)

9. 4 Mar 08Feng 9 The amount of dark matter left over is inversely proportional to the annihilation cross section:  DM ~  What is the constant of proportionality? Impose a natural relation:     k  2 /m 2, so  DM  m 2 Remarkable “coincidence”:  DM ~ 0.1 for m ~ 100 GeV – 1 TeV HEPAP LHC/ILC Subpanel (2006) [band width from k = 0.5 – 2, S and P wave]

10. 4 Mar 08Feng 10 STABILITY This all assumes that the new particle is stable. Why should it be? New Particle States Standard Model Particles Stable

11. 4 Mar 08Feng 11 PRECISION CONSTRAINTS Problem: Large Electron Positron Collider, 1989-2000, provided precision constraints on new particles new particle Higgs Good: Naturalness SM new particle Bad: Precision Constraints Solution: discrete parity  new particles interact in pairs. Lightest new particle is then stable. Cheng, Low (2003); Wudka (2003) Dark Matter is easier to explain than no dark matter.

12. 4 Mar 08Feng 12 Dark Matter! Propose Discrete Symmetry Find Problems Evaluate Precision Constraints Make a Model Predict DM Signals The WIMP paradigm is thriving. Examples: Supersymmetry –R-parity  Neutralino DM Goldberg (1983); Ellis et al. (1984) Universal Extra Dimensions –KK-parity  Kaluza-Klein DM Servant, Tait (2002); Cheng, Feng, Matchev (2002) Branes –Brane-parity  Branon DM Cembranos, Dobado, Maroto (2003) Little Higgs –T-parity  T-odd DM Cheng, Low (2003) PROLIFERATION OF WIMPS

13. 4 Mar 08Feng 13 WIMPS FROM SUPERSYMMETRY Goldberg (1983); Ellis et al. (1983) Supersymmetry: many motivations. For every known particle X, predicts a partner particle X̃ Neutralino   (  ̃, Z̃, H̃ u, H̃ d ) In many models,  is the lightest supersymmetric particle, stable, neutral, weakly-interacting, mass ~ 100 GeV. All the right properties for WIMP dark matter. In these scenarios, the LHC will see SUSY soon after beginning in 2008-09.

14. 4 Mar 08Feng 14 LARGE HADRON COLLIDER LHC: E COM = 14 TeV, 10 7 -10 9 top quarks/yr [Tevatron: E COM = 2 TeV, 10 2 -10 4 top quarks/yr]

15. 4 Mar 08Feng 15 LHC ATLAS Drawings Reality

16. 4 Mar 08Feng 16 WHAT THEN? What LHC actually sees: – E.g., q̃q̃ pair production – Each q̃  neutralino  – 2  ’s escape detector – missing momentum This is not the discovery of dark matter –Lifetime > 10 -7 s  10 17 s?

17. 4 Mar 08Feng 17 THE EXAMPLE OF BBN Nuclear physics  light element abundance predictions Compare to light element abundance observations Agreement  we understand the universe back to T ~ 1 MeV t ~ 1 sec

18. 4 Mar 08Feng 18 DARK MATTER ANALOGUE (1) (2) (3) Particle physics  dark matter abundance prediction Compare to dark matter abundance observation How well can we do?

19. 4 Mar 08Feng 19 Contributions to Neutralino WIMP Annihilation Jungman, Kamionkowski, Griest (1995)

20. 4 Mar 08Feng 20 PRECISION SUSY @ LHC Masses can be measured by reconstructing the decay chains Weiglein et al. (2004)

21. 4 Mar 08Feng 21 PRECISION SUSY @ ILC Collides e + e - Variable beam energies Polarizable e - beam Starts 20?? International Linear Collider ≈ ≈

22. 4 Mar 08Feng 22 WMAP (current) Planck (~2010) LHC (“best case scenario”) ILC LCC1 RELIC DENSITY DETERMINATIONS % level comparison of predicted  collider with observed  cosmo ALCPG Cosmology Subgroup

23. 4 Mar 08Feng 23 IDENTIFYING DARK MATTER Are  collider and  cosmo identical? Congratulations! You’ve discovered the identity of dark matter and extended our understanding of the Universe to T=10 GeV, t=1 ns (Cf. BBN at T=1 MeV, t=1 s) Yes Calculate the new  hep Can you discover another particle that contributes to DM? Which is bigger? No  collider  cosmo Does it account for the rest of DM? Yes No Did you make a mistake? Does it decay? Can you identify a source of entropy production? No Yes No Yes Can this be resolved with some non- standard cosmology? Yes No Are you sure? Yes Think about dark energy No

24. 4 Mar 08Feng 24 DARK ENERGY Freezeout provides a window on the very early universe: Probe Friedmann at T ~ 10 GeV: n=0 to 8: cosmological constant, tracking dark energy, quintessence, varying G N, … Drees, Iminniyaz, Kakizaki (2007) Chung, Everett, Kong, Matchev (2007) Dilution from expansion Carroll, Feng, Hsu (2008)

25. 4 Mar 08Feng 25 DIRECT DETECTION WIMP properties: v ~ 10 -3 c Kinetic energy ~ 100 keV Local density ~ 1 / liter Detected by recoils off ultra- sensitive underground detectors Theory predictions vary, but many* SUSY models  10 -44 cm *mSUGRA, focus point, gaugino-mediated, more minimal, 2-1 models, split SUSY, …

26. 4 Mar 08Feng 26 Future Direct Detection HEPAP/AAAC DMSAG Subpanel (2007)

27. 4 Mar 08Feng 27 DIRECT DETECTION IMPLICATIONS LHC + ILC   m < 1 GeV,  < 20% Comparison tells us about local dark matter density and velocity profiles, ushers in the age of neutralino astronomy

28. 4 Mar 08Feng 28 HESS COLLIDERS ELIMINATE PARTICLE PHYSICS UNCERTAINTIES, ALLOW ONE TO PROBE ASTROPHYSICAL DISTRIBUTIONS Particle Physics Astro- Physics Very sensitive to halo profiles near the galactic center INDIRECT DETECTION IMPLICATIONS

29. 4 Mar 08Feng 29 TAKING STOCK WIMPs are astrophysically identical –Weakly-interacting –Cold –Stable Is this true of all DM candidates? No. But is this true of all DM candidates independently motivated by particle physics and the “WIMP miracle”? No! SuperWIMPs: identical motivations, but qualitatively different implications

30. 4 Mar 08Feng 30 SUPERWIMPS: BASIC IDEA G̃ not LSP Assumption of most of literature SM LSP G̃G̃ G̃ LSP Completely different cosmology and particle physics SM NLSP G̃G̃ Supersymmetry: Graviton  Gravitino G̃ Mass ~ 100 GeV; Interactions: only gravitational (superweak) Feng, Rajaraman, Takayama (2003)

31. 4 Mar 08Feng 31 Suppose gravitinos G̃ are the LSP WIMPs freeze out as usual But then all WIMPs decay to gravitinos after M Pl 2 /M W 3 ~ seconds to months SUPERWIMP RELICS Gravitinos naturally inherit the right density, but interact only gravitationally – they are superWIMPs (also KK gravitons, quintessinos, axinos, etc.) G̃G̃ WIMP ≈ Feng, Rajaraman, Takayama (2003); Bi, Li, Zhang (2003); Ellis, Olive, Santoso, Spanos (2003); Wang, Yang (2004); Feng, Su, Takayama (2004); Buchmuller, Hamaguchi, Ratz, Yanagida (2004); Roszkowski, Ruiz de Austri, Choi (2004); Brandeburg, Covi, Hamaguchi, Roszkowski, Steffen (2005); …

32. 4 Mar 08Feng 32 Charged Particle Trapping SuperWIMPs are produced by decays of metastable particles. These can be charged. Charged metastable particles will be obvious at colliders, can be trapped and moved to a quiet environment to study their decays. Can catch 1000 per year in a 1m thick water tank Feng, Smith (2004) Hamaguchi, Kuno, Nakawa, Nojiri (2004) De Roeck et al. (2005) Charged particle trap Reservoir

33. 4 Mar 08Feng 33 IMPLICATIONS FROM CHARGED PARTICLE DECAYS Measurement of  m l ̃ and E l  m G̃ and G N –Probes gravity in a particle physics experiment! –Measurement of G N on fundamental particle scale –Precise test of supergravity: gravitino is graviton partner –Determines  G̃ : SuperWIMP contribution to dark matter –Determines F : supersymmetry breaking scale, contribution of SUSY breaking to dark energy, cosmological constant Hamaguchi et al. (2004); Takayama et al. (2004)

34. 4 Mar 08Feng 34 SUPERWIMP COSMOLOGY Late decays can modify CMB black body spectrum (  distortions) Fields, Sarkar, PDG (2002) Late decays can modify BBN (Resolve 6,7 Li problems?) Fixsen et al. (1996)

35. 4 Mar 08Feng 35 SuperWIMPs are produced in late decays with large velocity (0.1c – c) Suppresses small scale structure, as determined by FS, Q Warm DM with cold DM pedigree SMALL SCALE STRUCTURE Dalcanton, Hogan (2000) Lin, Huang, Zhang, Brandenberger (2001) Sigurdson, Kamionkowski (2003) Profumo, Sigurdson, Ullio, Kamionkowski (2004) Kaplinghat (2005) Cembranos, Feng, Rajaraman, Takayama (2005) Strigari, Kaplinghat, Bullock (2006) Bringmann, Borzumati, Ullio (2006) Kaplinghat (2005) Sterile Dodelson, Widrow (1993) SuperWIMP

36. 4 Mar 08Feng 36 CONCLUSIONS Particle Dark Matter –As well-motivated as ever –WIMPs: Proliferation of candidates –SuperWIMPs: Qualitatively new possibilities (warm, metastable, only gravitationally interacting) If dark matter is WIMPs or superWIMPs, colliders –will produce it –may identify it as dark matter –may open up a window on the universe at t ~ 1 ns LHC begins in 08-09, direct and indirect detection are improving rapidly – this field will be transformed soon